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2023-01-16T05:03:56Z
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Magnetohydrodynamic Simulations for Studying Solar Flare Trigger Mechanism
Muhamad, J.
73592
Kusano, K.
73593
Inoue, S.
73594
Shiota, D.
73595
magnetohydrodynamics (MHD)
Sun: activity
Sun: corona
Sun: magnetic fields
In order to understand the flare trigger mechanism, we conduct three-dimensional magnetohydrodynamic simulations using a coronal magnetic field model derived from data observed by the Hinode satellite. Several types of magnetic bipoles are imposed into the photospheric boundary of the Nonlinear Force-free Field model of Active Region (AR) NOAA 10930 on 2006 December 13, to investigate what kind of magnetic disturbance may trigger the flare. As a result, we confirm that certain small bipole fields, which emerge into the highly sheared global magnetic field of an AR, can effectively trigger a flare. These bipole fields can be classified into two groups based on their orientation relative to the polarity inversion line: the so-called opposite polarity, and reversed shear structures, as suggested by Kusano et al. We also investigate the structure of the footpoints of reconnected field lines. By comparing the distribution of reconstructed field lines and observed flare ribbons, the trigger structure of the flare can be inferred. Our simulation suggests that the data-constrained simulation, taking into account both the large-scale magnetic structure and small-scale magnetic disturbance (such as emerging fluxes), is a good way to discover a flare-producing AR, which can be applied to space weather prediction.
journal article
IOP publishing
2017-06-20
application/pdf
The Astrophysical Journal
2
842
86
86
http://doi.org/10.3847/1538-4357/aa750e
http://hdl.handle.net/2237/26982
0004-637X
https://nagoya.repo.nii.ac.jp/record/24760/files/pdf.pdf
eng
https://doi.org/10.3847/1538-4357/aa750e
© 2017 The American Astronomical Society